scholarly journals Argon Abundances in the Solar Neighborhood: Non‐LTE Analysis of Orion Association B‐Type Stars1

2008 ◽  
Vol 678 (2) ◽  
pp. 1342-1350 ◽  
Author(s):  
Thierry Lanz ◽  
Katia Cunha ◽  
Jon Holtzman ◽  
Ivan Hubeny
Keyword(s):  
Solar Neighborhood ◽  
Orion Association

A Search for Dyson Spheres around Late-Type Stars in the Solar Neighborhood II

1997 ◽  
Vol 161 ◽  
pp. 707-709 ◽  
Author(s):  
Jun Jugaku ◽  
Shiro Nishimura
Keyword(s):  
Solar Neighborhood ◽  
The Sun ◽  
Late Type ◽  
Solar Type

AbstractWe continued our search for partial (incomplete) Dyson spheres associated with 50 solar-type stars (spectral classes F, G, and K) within 25 pc of the Sun. No candidate objects were found.

Boron Abundances of B Stars of the Orion Association

1997 ◽  
Vol 478 (1) ◽  
pp. 211-224 ◽  
Author(s):  
Katia Cunha ◽  
David L. Lambert ◽  
Michael Lemke ◽  
Douglas R. Gies ◽  
Lewis C. Roberts
Keyword(s):  
B Stars ◽  
Orion Association

Chemical Evolution of the Orion Association. IV. The Oxygen and Iron Abundances of F and G Stars

1998 ◽  
Vol 493 (1) ◽  
pp. 195-205 ◽  
Author(s):  
Katia Cunha ◽  
Verne V. Smith ◽  
David L. Lambert
Keyword(s):  
Chemical Evolution ◽  
Orion Association

scholarly journals Abundances in the Gaseous Galactic Halo

1998 ◽  
Vol 11 (1) ◽  
pp. 86-89
Author(s):  
Ulysses J. Sofia
Keyword(s):  
Interstellar Medium ◽  
Gas Phase ◽  
High Velocity ◽  
Galactic Halo ◽  
Solar Neighborhood ◽  
Local Interstellar Medium ◽  
The Galaxy ◽  
Metal Abundances ◽  
High Velocity Clouds

Abstract The well measured gas-phase abundances in the low halo suggest that this region of the Galaxy has total (gas plus dust) metal abundances which are close to those in the solar neighborhood. The gas-phase abundances in the halo are generally higher than those seen in the disk, however, this affect is likely due to the destruction of dust in the halo clouds. Observations of high velocity clouds (HVCs) in the halo suggest that these clouds have metal abundances which are substantially lower than those measured for the local interstellar medium. These determinations, however, are often of lower quality than those for the low halo because of uncertainties in the hydrogen abundances along the sightlines, in the incorporation of elements into dust, and in the partial ionization of the clouds.

scholarly journals The Solar Neighborhood. XLV. The Stellar Multiplicity Rate of M Dwarfs Within 25 pc

2019 ◽  
Vol 157 (6) ◽  
pp. 216 ◽  
Author(s):  
Jennifer G. Winters ◽  
Todd J. Henry ◽  
Wei-Chun Jao ◽  
John P. Subasavage ◽  
Joseph P. Chatelain ◽  
...  
Keyword(s):  
Solar Neighborhood ◽  
M Dwarfs

scholarly journals Contribution of White Dwarfs to Cluster Masses

1998 ◽  
Vol 11 (1) ◽  
pp. 430-432
Author(s):  
Ted Von Hippel
Keyword(s):  
Stellar Evolution ◽  
Mass Fraction ◽  
Globular Clusters ◽  
White Dwarfs ◽  
Literature Search ◽  
Galactic Disk ◽  
Dynamical Evolution ◽  
Open Clusters ◽  
Solar Neighborhood ◽  
Current Evidence

The study of cluster white dwarfs (WDs) has been invigorated recently bythe Hubble Space Telescope (HST). Recent WD studies have been motivated by the new and independent cluster distance (Renzini et al. 1996), age (von Hippel et al. 1995; Richer et al. 1997), and stellar evolution (Koester & Reimers 1996) information that cluster WDs can provide. An important byproduct of these studies has been an estimate of the WD mass contribution in open and globular clusters. The cluster WD mass fraction is of importance for understanding the dynamical state and history of star clusters. It also bears an important connection to the WD mass fractions of the Galactic disk and halo. Current evidence indicates that the open clusters (e.g. von Hippel et al. 1996; Reid this volume) have essentially the same luminosity function (LF) as the solar neighborhood population. The case for the halo is less clear, despite the number of very good globular cluster LFs down to nearly 0.1 solar masses (e.g. Cool et al. 1996; Piotto, this volume), as the field halo LF is poorly known. For most clusters dynamical evolution should cause evaporation of the lowest mass members, biasing clusters to have flatter present-day mass functions (PDMFs) than the disk and halo field populations. Dynamical evolution should also allow cluster WDs to escape, though not in the same numbers as the much lower mass main sequence stars. The detailed connection between cluster PDMFs and the field IMF awaits elucidation from observations and the new combined N-body and stellar evolution models (Tout, this volume). Nevertheless, the WD mass fraction of clusters already provides an estimate for the WD mass fraction of the disk and halo field populations. A literature search to collect cluster WDs and a simple interpretive model follow. This is a work in progress and the full details of the literature search and the model will be published elsewhere.

Observations of White Dwarfs in the Solar Neighborhood

2004 ◽  
Vol 127 (3) ◽  
pp. 1702-1711 ◽  
Author(s):  
Adela Kawka ◽  
Stphane Vennes ◽  
John R. Thorstensen
Keyword(s):  
White Dwarfs ◽  
Solar Neighborhood

scholarly journals THE SOLAR NEIGHBORHOOD. XXX. FOMALHAUT C

2013 ◽  
Vol 146 (6) ◽  
pp. 154 ◽  
Author(s):  
Eric E. Mamajek ◽  
Jennifer L. Bartlett ◽  
Andreas Seifahrt ◽  
Todd J. Henry ◽  
Sergio B. Dieterich ◽  
...  
Keyword(s):  
Solar Neighborhood

scholarly journals The Solar Neighborhood. XVIII. Discovery of New Proper-Motion Stars with 0.40" yr-1> μ ≥ 0.18" yr-1between Declinations -90° and -47°

2007 ◽  
Vol 133 (6) ◽  
pp. 2898-2907 ◽  
Author(s):  
Charlie T. Finch ◽  
Todd J. Henry ◽  
John P. Subasavage ◽  
Wei-Chun Jao ◽  
Nigel C. Hambly
Keyword(s):  
Proper Motion ◽  
Solar Neighborhood
Sign in / Sign up

Export Citation Format

Share Document